Changes between Version 33 and Version 34 of GravoTurbulence

Timestamp:

12/15/11 18:09:52 (13 years ago)

Author:

Jonathan

Comment:

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GravoTurbulence

@@ -114 +114 @@
 
 
-Unless the dense blobs are gravitationally confined.  But how to go from a power spectra of density fluctuations to a mass-size relation?  We have [[latex($\hat{\rho}(\mathbf{k}) \propto \exp^{A|k|^{\beta}}$)]]?  If [[latex($k << \lambda_k = c_s\sqrt{\frac{\pi}{G}} \rho^{-1/2}$)]] then the fluctuations should be jeans unstable - but \rho = }
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+Unless the dense blobs are gravitationally confined.  But how to go from a power spectra of density fluctuations to a mass-size relation?  We have [[latex($\hat{\rho}(\mathbf{k}) \propto \rho_0\exp^{A|k|^{\beta}}$)]]?  If [[latex($k << \lambda_k = c_s\sqrt{\frac{\pi}{G}} \rho^{-1/2}$)]] then the fluctuations should be jeans unstable - but [[latex($\rho(k) = \displaystyle{\int_{k_{min}}^k{\hat{\rho}(\mathbf{k}) \mathbf{dk^3}}}$)]].  If we consider the largest scales only, then [[latex($k_{min} << c_s\sqrt{\frac{\pi}{G}} \left( \rho_0 \exp(A k_{min}) \right )^{-1/2}$)]]